Super-Eddington accretion discs with 3 and 15 \dot { M } _ { E } around black holes with mass 10 M _ { \odot } are examined by two-dimensional radiation hydrodynamical calculations extending from the inner disc edge to 5 \times 10 ^ { 4 } r _ { g } and lasting up to \sim 10 ^ { 6 } r _ { g } / c .
The dominant radiation-pressure force in the inner region of the disc accelerates the gas vertically to the disc plane , and jets with 0.2 – 0.4 c are formed along the rotational axis .
In the case of the lower accretion rate , the initially anisotropic high-velocity jet expands outward and becomes gradually isotropic flow in the distant region .
The mass-outflow rate from the outer boundary is as large as \sim 10 ^ { 19 } – 10 ^ { 23 } g s ^ { -1 } , but it is variable and intermittent with time ; that is , the outflow switches occasionally to inflow in the distant region .
The luminosity also varies as \sim 10 ^ { 40 } – 10 ^ { 42 } erg s ^ { -1 } on a long time-scale .
On the other hand , the jet in the case of the higher accretion rate maintains its initial anisotropic shape even after it goes far away .
The mass-outflow rate and the luminosity attain to steady values of 3 \times 10 ^ { 19 } g s ^ { -1 } and 1.3 \times 10 ^ { 40 } erg s ^ { -1 } , respectively .
In accordance with the local analysis of the slim accretion disc model , the disc is thermally unstable in the case of 3 \dot { M } _ { E } but stable in the case of 15 \dot { M } _ { E } .
The super-Eddington model with 15 \dot { M } _ { E } is promising to explain a small collimation degree of the jet and a large mass-outflow rate observed in the X-ray source SS 433 .